THE SPITZER–WISE SURVEY OF THE ECLIPTIC POLES

By Thomas H. Jarrett, M. Cohen, F. Masci, E. L. Wright, Daniel Stern, Dominic J. Benford, A. Blain, S. Carey, R. Cutri, P. Eisenhardt and 12 more. 2011

438 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9d653fd7ced2688bc75a0cf578aeb873fe6e42c8

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Citations in the corpus

The Absolute Magnitude of the Sun in Several Filters (2018, neutral): “…8: Hewett et al. (2006); 9: https://github.com/lsst/throughputs/tree/master/baseline 10: Bessell & Murphy (2012); 11: Bessell & Brett (1988); 12: GSFC (2012); 13: Jarrett et al. (2011); 14: Gillett et al. (1984); 15: NASA/IPAC Infrared Science Archive (2010); 15: STScI (2017a); 16: STScI (2017b).”
IDENTIFICATION OF 1.4 MILLION ACTIVE GALACTIC NUCLEI IN THE MID-INFRARED USING WISE DATA (2015, methodology): “…Spitzer two-color criteria in Lacy et al. (2004), Stern et al. (2005), Lacy et al. (2007), and Donley et al. (2012); the WISE two-color criteria in Jarrett et al. (2011), the WISE one-color criteria of Stern et al. (2012) and Assef et al. (2013), and the WISE two-color criteria of Mateos et al.…”
TWO MICRON ALL SKY SURVEY PHOTOMETRIC REDSHIFT CATALOG: A COMPREHENSIVE THREE-DIMENSIONAL CENSUS OF THE WHOLE SKY (2013, background): “In addition, issues are being raised regarding the SFD maps in general, for instance that they may overestimate the extinction over the entire sky, not only in the Galactic Plane (Schlafly & Finkbeiner 2011; Yuan et al. 2013) and new dust maps are currently in development, in particular with the use”
MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER. II. PROPERTIES OF WISE-SELECTED ACTIVE GALACTIC NUCLEI IN THE NDWFS BOÖTES FIELD (2012, background): “While fields near the ecliptic were typically observed 12 times, the number can grow to several hundreds near the ecliptic poles (e.g., Jarrett et al. 2011).”
The Sloan Digital Sky Survey quasar catalog: ninth data release (2012, methodology): “Formulae for converting WISE Vega magnitudes to flux density units (in Janskys) and AB magnitudes are given in Wright et al. (2010) and Jarrett et al. (2011) and also here: http://wise2.ipac.caltech.edu/docs/release/- allsky/expsup/sec44h.html#conv2flux Although the MIR WISE properties of the BOSS…”
Galaxy Interactions Trigger Rapid Black Hole Growth: an unprecedented view from the Hyper Suprime-Cam Survey (2017, methodology): “…mid-IR photometry taken using the IRAC instrument on the NASA Spitzer Space Telescope (e.g., Lacy et al. 2004; Stern et al. 2005; AlonsoHerrero et al. 2006; Donley et al. 2012, or more recently using WISE (e.g., Jarrett et al. 2011; Stern et al. 2012; Mateos et al. 2012), which we harness here.”
Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey (2014, background): “The third correction comes from a discrepancy between the WISE photometric standard “blue” stars and “red” galaxies related to an error in the W4 RSR, as described in Wright et al. (2010) and Jarrett et al. (2011).”
CHARACTERIZING THE MID-INFRARED EXTRAGALACTIC SKY WITH WISE AND SDSS (2012, methodology): “The conversion factors to the AB system (mAB ≡ mVega + ∆m) are 2.683 (W1), 3.319 (W2), 5.242 (W3) and 6.604 (W4); equivalently, zero magnitude corresponds to 309.5, 171.79, 31.676 and 8.36 Jy for the four bands, respectively (Wright et al. 2010) and (Jarrett et al. 2011).”
MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER. I. CHARACTERIZING WISE-SELECTED ACTIVE GALACTIC NUCLEI IN COSMOS (2012, background): “Higher latitude fields have deeper data, reaching a coverage of 250 frames at the ecliptic poles (Jarrett et al. 2011).”
HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, methodology): “Photometric magnitudes were converted to fluxes using the zero points from Cohen et al. (2003) for 2MASS, Jarrett et al. (2011) for WISE, and Mann & von Braun (2015) for all other photometry.”
AN ATLAS OF GALAXY SPECTRAL ENERGY DISTRIBUTIONS FROM THE ULTRAVIOLET TO THE MID-INFRARED (2013, methodology): “The WISE photometric measurements are calibrated using a network of A stars and K-M giants (Jarrett et al. 2011), with typical spectral indices (α) between 1 and 2, where the spectral index is defined by fν ∝ ν α.”
INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, methodology): “Similarly, for the WISE bands we use RSR curves available on the IPAC website6 with the zero magnitude flux given in Jarrett et al. (2011).”
EXTENDING THE NEARBY GALAXY HERITAGE WITH WISE: FIRST RESULTS FROM THE WISE ENHANCED RESOLUTION GALAXY ATLAS (2012, methodology): “Based on work summarized in Jarrett et al. (2011), we have adopted a factor of 0.92 correction to the W4 flux of all of our galaxies, except those dominated by the old stellar population (NGC 584, NGC 777, M 87 and NGC 6822) in which case no flux correction is needed.”
GALAXY AND MASS ASSEMBLY (GAMA): MID-INFRARED PROPERTIES AND EMPIRICAL RELATIONS FROM WISE (2014, methodology): “The work of Donoso et al. (2012) showed the power of combining WISE with a large-area survey (SDSS); they investigated the effect of star formation- and AGN-activity on the WISE properties of >95,000 galaxies, including calibrations using the 12 μm and 22 μm luminosities.”
The WISE AGN Catalog (2017, background): “As noted by Jarrett et al. (2011), requiring a detection in W3 can be particularly useful near the high survey coverage areas at the ecliptic poles, where the W1 and W2 are confusion limited, and the lower source density W3 band provides robust photometry.”